The Rave Catalog of Stellar Elemental Abundances: First Data Release

Boeche, C.; Siebert, A.; Williams, M.; Jong, Roelof S. de; Steinmetz, Matthias; Fulbright, Jon P.; Ruchti, G.; Bienaymé, O.; Bland-Hawthorn, Joss; Campbell, Randy; Freeman, K. C.; Gibson, Brad K.; Gilmore, G.; Grebel, Eva K.; Helmi, Amina; Munari, U.; Navarro, Julio F.; Parker, Quentin A.; Reid, Warren A.; Seabroke, G. M.; Siviero, A.; Watson, Fred; Wyse, Rosemary F. Ġ.; Zwitter, T.

doi:10.1088/0004-6256/142/6/193

Cited by 83 publications

(109 citation statements)

References 46 publications

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“…Systematic abundance offsets of 0.2 to 0.3 dex between equivalent width measurements and χ 2 minimisation techniques (in the sense that the χ 2 minimisation gives lower abundances) have also been reported by the RAVE survey team (Zwitter et al 2008;Boeche et al 2011), in particular for giant stars. No explanation as for the possible origin of this offset is given in the literature, neither did we attempt to track down its cause.…”

Section: Systematic Errorsmentioning

confidence: 58%

Constraining the structure and formation of the Galactic bulge from a field in its outskirts

Uttenthaler¹,

Schultheis²,

Nataf³

et al. 2012

A&A

133

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Context. The presence of two stellar populations in the Milky Way bulge has been reported recently, based on observations of giant and dwarf stars in the inner and intermediate bulge.Aims. We aim at studying the abundances and kinematics of stars in the outer Galactic bulge, thereby providing additional constraints on formation models of the bulge. Methods. Spectra of 401 red giant stars in a field at (l, b) = (0 • , −10 • ) were obtained with the FLAMES-GIRAFFE spectrograph at the VLT. Stars of luminosities down to below the two bulge red clumps are included in the data set. From these spectra we measured general metallicities, abundances of iron and the α-elements, and radial velocities of the stars. The abundances were derived from an interpolation and fitting procedure within a grid of COMARCS model atmospheres and spectra. These measurements as well as photometric data were compared to simulations with the Besançon and TRILEGAL models of the Galaxy. Results. We confirm the presence of two populations among our sample stars: i) a metal-rich one at [M/H] ∼ +0.3, comprising about 30% of the sample, with low velocity dispersion and low α-abundance, and ii) a metal-poor population at [M/H] ∼ −0.6 with high velocity dispersion and high α-abundance. The metallicity difference between the two populations, a systematically and statistically robust figure, is Δ[M/H] = 0.87 ± 0.03. The metal-rich population could be connected to the Galactic bar. We identify this population as the carrier of the double red clump feature. We do not find a significant difference in metallicity or radial velocity between the two red clumps, a small difference in metallicity being probably due to a selection effect and contamination by the metal-poor population. The velocity dispersion agrees well with predictions of the Besançon Galaxy model, but the metallicity of the "thick bulge" model component should be shifted to lower metallicity by 0.2 to 0.3 dex to well reproduce the observations. We present evidence that the metallicity distribution function depends on the evolutionary state of the sample stars, suggesting that enhanced mass loss preferentially removes metal-rich stars. We also confirm the decrease of α-element over-abundance with increasing metallicity. Conclusions. Our sample is consistent with the existence of two populations, one being a metal-rich bar, the second one being more like a metal-poor classical bulge with larger velocity dispersion.

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Section: Systematic Errorsmentioning

confidence: 58%

Constraining the structure and formation of the Galactic bulge from a field in its outskirts

Uttenthaler¹,

Schultheis²,

Nataf³

et al. 2012

A&A

133

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“…19 (Boeche et al 2011). The RAVE [M/H] accuracy is apparently not high enough to carry out a detailed metallicity study within OCs.…”

Section: Metallicitymentioning

confidence: 99%

“…To verify this hypothesis we analysed the results of the chemical pipeline implemented for RAVE by Boeche et al (2011). These authors employed slightly more stringent quality constraints (S/N ≥ 20, v rot < 50 km s −1 and 4000 < T eff < 7000 K).…”

Section: Metallicitymentioning

confidence: 99%

A RAVE investigation on Galactic open clusters

Conrad

Scholz

Kharchenko

et al. 2017

A&A

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“…The conversion between the extinction in the optical and near-IR wavelength range is performed following Rieke & Lebofsky (1985). We adopted the [Fe/H] and [α/Fe] estimates from the chemical RAVE pipeline (Boeche et al 2011;Kordopatis et al 2013) to make our metallicity scale more compatible with the stellar models, as in the previous sections.…”

Section: Ravementioning

confidence: 99%

Spectro-photometric distances to stars: A general purpose Bayesian approach

Santiago

Brauer

Anders

et al. 2015

A&A

108

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Context. Determining distances to individual field stars is a necessary step towards mapping Galactic structure and determining spatial variations in the chemo-dynamical properties of stellar populations in the Milky Way. Aims. In order to provide stellar distance estimates for various spectroscopic surveys, we have developed a code that estimates distances to stars using measured spectroscopic and photometric quantities. We employ a Bayesian approach to build the probability distribution function over stellar evolutionary models given these data, delivering estimates of model parameters (including distances) for each star individually. Our method provides several alternative distance estimates for each star in the output, along with their associated uncertainties. This facilitates the use of our method even in the absence of some measurements. Methods. The code was first tested on simulations, successfully recovering input distances to mock stars with 1% bias. We found the uncertainties scale with the uncertainties in the adopted spectro-photometric parameters. The method-intrinsic random distance uncertainties for typical spectroscopic survey measurements amount to around 10% for dwarf stars and 20% for giants, and are most sensitive to the quality of log g measurements. Results. The code was then validated by comparing our distance estimates to parallax measurements from the H mission for nearby stars (<300 pc), to asteroseismic distances of CoRoT red giant stars, and to known distances of well-studied open and globular clusters. The photometric data of these reference samples cover both optical and infrared wavelengths. The spectroscopic parameters are also based on spectra taken at various wavelengths, with varying spectral coverage and resolution: the Sloan Digital Sky Survey programs SEGUE and APOGEE, as well as various ESO instruments. Conclusions. External comparisons confirm that our distances are subject to very small systematic biases with respect to the fundamental H scale (+0.4% for dwarfs, and +1.6% for giants). The typical random distance scatter is 18% for dwarfs, and 26% for giants. For the CoRoT-APOGEE sample, which spans Galactocentric distances of 4−14 kpc, the typical random distance scatter is 15% both for the nearby and farther data. Our distances are systematically larger than the CoRoT distances by about +9%, which can mostly be attributed to the different choice of priors. The comparison to known distances of star clusters from SEGUE and APOGEE has led to significant systematic differences for many cluster stars, but with opposite signs and substantial scatter. Finally, we tested our distances against those previously determined for a high-quality sample of giant stars from the RAVE survey, again finding a small systematic trend of +5% and an rms scatter of 30%. Efforts are underway to provide our code to the community by running it on a public server.

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The Rave Catalog of Stellar Elemental Abundances: First Data Release

Cited by 83 publications

References 46 publications

Constraining the structure and formation of the Galactic bulge from a field in its outskirts

Constraining the structure and formation of the Galactic bulge from a field in its outskirts

A RAVE investigation on Galactic open clusters

Spectro-photometric distances to stars: A general purpose Bayesian approach

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